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An Updated Type II Supernova Hubble Diagram? A&A 611, A25 (2018) Astronomy DOI: 10.1051/0004-6361/201731271 & c ESO 2018 Astrophysics An updated Type II supernova Hubble diagram? E. E. E. Gall1; 2, R. Kotak1, B. Leibundgut3; 4, S. Taubenberger2; 3, W. Hillebrandt2, M. Kromer5; 6; 7, W. S. Burgett8, K. Chambers9, H. Flewelling9, M. E. Huber9, N. Kaiser9, R. P. Kudritzki9, E. A. Magnier9, N. Metcalfe10, K. Smith1, J. L. Tonry9, R. J. Wainscoat9, and C. Waters9 1 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK e-mail: [email protected] 2 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching-bei-München, Germany 3 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany 4 Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching-bei-München, Germany 5 Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany 6 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Philosophenweg 12, 69120 Heidelberg, Germany 7 The Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden 8 GMTO Corporation, 465 N. Halstead St., Suite 250 Pasadena, CA 91107, USA 9 Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 10 Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK Received 30 May 2017 / Accepted 9 October 2017 ABSTRACT We present photometry and spectroscopy of nine Type II-P/L supernovae (SNe) with redshifts in the 0:045 . z . 0:335 range, with a view to re-examining their utility as distance indicators. Specifically, we apply the expanding photosphere method (EPM) and the standardized candle method (SCM) to each target, and find that both methods yield distances that are in reasonable agreement with each other. The current record-holder for the highest-redshift spectroscopically confirmed supernova (SN) II-P is PS1-13bni +0:009 (z = 0:335−0:012), and illustrates the promise of Type II SNe as cosmological tools. We updated existing EPM and SCM Hubble diagrams by adding our sample to those previously published. Within the context of Type II SN distance measuring techniques, we investigated two related questions. First, we explored the possibility of utilising spectral lines other than the traditionally used Fe ii λ5169 to infer the photospheric velocity of SN ejecta. Using local well-observed objects, we derive an epoch-dependent relation between the strong Balmer line and Fe ii λ5169 velocities that is applicable 30 to 40 days post-explosion. Motivated in part by the continuum of key observables such as rise time and decline rates exhibited from II-P to II-L SNe, we assessed the possibility of using Hubble-flow Type II-L SNe as distance indicators. These yield similar distances as the Type II-P SNe. Although these initial results are encouraging, a significantly larger sample of SNe II-L would be required to draw definitive conclusions. Key words. supernovae: general – distance scale 1. Introduction indicators, calibrated using Cepheid distances, they reported a −1 −1 value for H0 of 72 ± 8 km s Mpc . The past decades have been marked by an ongoing revolution in Galaxies for which distance estimates from multiple sources cosmology and distance estimation techniques. Following the as- are available are crucial as anchors for the extragalactic distance tounding discovery that the Universe was expanding at an accel- scale. One example is NGC 4258, which has estimates for a ge- erating rate (Riess et al. 1998; Perlmutter et al. 1999), the quest ometric distance through mega masers (Humphreys et al. 2013), to determine the precise value of the Hubble constant, H , has 0 a Cepheid distance (e.g. Fiorentino et al. 2013), and a Type II-P inspired a host of new distance determination techniques, sys- supernova (SN) distance (Polshaw et al. 2015). NGC 4258 may tematic improvements to old approaches, as well as large-scale therefore be a more suitable anchor galaxy than the Large Magel- focussed projects dedicated to improving the precision in the lanic Cloud, which was used as the first rung on the distance lad- measurements of H in order to shed light on the constituents 0 der for a variety of distance estimation techniques (Riess et al. of the energy density of the Universe. 2011a,b, and references therein). Already in the 1980s i.e., before the launch of the Hubble Space Telescope (HST), the measurement of the Hubble con- Recently, the Planck Collaboration XIII(2016) presented the stant with an uncertainty of .10% was chosen as one of three outcomes of observations of the cosmic microwave background, = HST “Key Projects”. Freedman et al.(2001) presented the final which enabled them to restrict the Hubble constant to H0 ± −1 −1 results of this endeavour. Using an array of secondary distance 67.8 0.9 km s Mpc , corresponding to an uncertainty of only 1.3%. ? Tables A.1, A.3, A.5, A.7, A.9, A.11, A.13, A.15 and A.17 are also In the latest update, Riess et al.(2016) combined both newly available at the CDS via anonymous ftp to calibrated distance measurements of Cepheid stars and Type Ia cdsarc.u-strasbg.fr (130.79.128.5) or via SNe, to constrain the Hubble constant to only 2.4% as H0 = http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/611/A25 73.0 ± 1.8 km s−1 Mpc−1. Article published by EDP Sciences A25, page 1 of 38 A&A 611, A25 (2018) While the uncertainties in H0 have decreased significantly redshifts, a subtlety that was neglected in previous studies. We over the years, a disagreement at the 2.0–2:5σ level between the re-derived the basic equations of the EPM, and showed that for values derived via SN Ia cosmology and measurements of the distant SNe, the angular size, θ, should be corrected by a factor cosmic microwave background has emerged, reflecting a tension of (1 + z)2, and that the observed flux has to be transformed into between local and global measurements of H0. Such a discrep- the SN rest frame. These findings were applied to SN 2013eq ancy could either imply unknown systematic uncertainties in the (z = 0.041 ± 0.001) in Gall et al.(2016), implementing both the measurements of H0 or that current cosmological models have to EPM and SCM, and demonstrated that the two techniques give be revised (e.g. Bennett et al. 2014). Nevertheless, Bennett et al. consistent results. (2014) also maintain that the various estimates of H0 are not in- However, even in the local Universe the division between consistent with each other. SNe II-P – which are typically used for the EPM and SCM The Expanding Photosphere Method (EPM; Kirshner & – and SNe II-L is ambiguous and has given rise to exten- Kwan 1974) and the Standardized Candle Method (SCM; sive discussions on whether SNe II-P/L should (Anderson et al. Hamuy & Pinto 2002) and their more recent derivatives pro- 2014; Sanders et al. 2015), or should not (Arcavi et al. 2012; vide independent routes to H0. On the most fundamental level, Faran et al. 2014) be viewed as members of the same class the EPM relies on the comparison of the angular size of with a continuum of properties. The rise times of a sample an object with the ratio between its observed and theoretical of 20 Type II-P and II-L SNe were analyzed in Gall et al. flux, whereas the SCM uses the relation between the expan- (2015), amongst them LSQ13cuw, a Type II-L SN with excel- sion velocities of SNe II-P during the plateau phase and its lent constraints on its explosion epoch (<1 d). We found some plateau luminosity to determine the distance. The EPM and evidence for SNe II-L having longer rise times and higher lumi- SCM are subject to different systematics than the previously nosities than SNe II-P, but also indications that a clear separa- mentioned techniques and they have both undergone signifi- tion of SNe II-P/L into two distinct classes can be challenging cant improvements from their original description (e.g. Wagoner (see also González-Gaitán et al. 2015; Rubin & Gal-Yam 2016). 1981; Schmidt et al. 1994b; Eastman et al. 1996; Hamuy et al. Given that this distinction is marginal, we investigate the possi- 2001; Dessart & Hillier 2005; Gall et al. 2016 for the EPM or bility of including SNe II-L into the Hubble diagram. Nugent et al. 2006; Poznanski et al. 2009 for the SCM), aim- We push the EPM and SCM techniques further, by apply- ing to reduce their systematic uncertainties. In particular, the ing both techniques to a set of Type II-P/L SNe, with redshifts EPM is independent of the cosmic distance ladder. Additionally, in the following range: 0:04 < z < 0:34. Three SNe in our SNe II-P are more common albeit less luminous than SNe Ia, sample exhibited post-peak decline rates that would be consis- and bear the potential to be observed in statistically significant tent with a Type II-L classification. This has little bearing on numbers. our results. Our sample also includes PS1-13bni with a red- +0:009 Several other methods have been proposed to either improve shift of z = 0:335−0:012 – to the best of our knowledge – the on EPM or reduce the observational effort, mostly spectroscopy, highest-redshift Type II-P SN discovered yet. We prepare the for distance determination with Type II SNe. The application path for future surveys that will find statistically significant num- of a single dilution factor for the black body radiation has bers of SNe II-P/L in the Hubble flow, and provide an indepen- been shown to be a clear limitation of EPM.
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